galactic cosmicray propagation in the ams02 era
TRANSCRIPT
![Page 1: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/1.jpg)
30/05/2012
I – Science case1. Galactic Cosmic Rays2. AMS02
II – Collaboration LAPP/LAPTh/LPSC1. Teams and context2. Support asked for the project
III – Conclusions
Galactic CosmicRay Propagation in the AMS02 Era
David [email protected]
ENIGMASS
(a few slides are borrowed from L. Derome and S. Rosier)
![Page 2: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/2.jpg)
Dark Matter annihilation products and flux
Dark MatterHalo
~ 300 kpc
~ 15 kpc
8 kpc
=> background for detection are all possible astrophysical contributions! p (CR) + H (ISM) → antiprotons, positrons, diffuse -rays...
=> same transport for DM or astrophysically-induced species i
![Page 3: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/3.jpg)
Particle transport: neutral and charged particles
~ 15 kpc
8 kpc
Neutral particles: - propagate in straight line- absorption ~ negligible at GeV-TeV in the Galaxy
=> line-of-sight integration on skymaps + spectra
Dark MatterHalo
~ 300 kpc
CLUMPY http://lpsc.in2p3.fr/clumpy/
![Page 4: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/4.jpg)
Particle transport: neutral and charged particles
Effectivevolume
for contributing
sources
~ 15 kpc
8 kpc
Neutral particles: - propagate in straight line- absortion ~ negligible at GeV-TeV in the Galaxy
=> line-of-sight integration on skymaps + spectra
Charge particles: - Diffusion (random walk) in magnetic fields- Continuous (energy) and catastrophic losses (destruction)
=> 'local' (~100 pc to a few kpc, depending on E)effective diffusive volume and isotropisation: single spectrum
Dark MatterHalo
~ 300 kpc
Radio (magnetic)
halo~ 10 kpc
USINE http://lpsc.in2p3.fr/usine/
CLUMPY http://lpsc.in2p3.fr/clumpy/
![Page 5: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/5.jpg)
F. Barao, R. Duperray
Matter
Anti-Matter
Neutral
Nuclei: H, He, CNO, Fe… - Light, heavy, VH and UH - Stable, and EC rad. Electons [e/p ~ 1% @ GeV]
Anti-nuclei: pbar, dbar…Positrons [e+/e- ~ 10%]
GeVTeV GCR spectra.
and
GCR content
- DM 'signal' as 'features' (or excess) in GCR spectra- Do we know well the expected astrophysical spectra?
=> Use 2H, 3He, LiBeB, sub-Fe to calibrate the transport
=> Search for DM where “standard” production is rare (secondary)
![Page 6: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/6.jpg)
AMS on ISS: 19th of May 2011
![Page 7: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/7.jpg)
White Sands Ground Terminal, NM
AMS Computers at MSFC, AL
AMS Payload Operations Control and Science Operations Centers
(POCC, SOC) at CERN
AMSTDRS Satellites
Astronaut at ISS AMS Laptop
Ku-BandHigh Rate (down):Events <10Mbit/s>
S-BandLow Rate (up & down):Commanding: 1 Kbit/sMonitoring: 30 Kbit/s
AMS data flow
![Page 8: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/8.jpg)
Events collected Events reconstructed
=> Several times the whole statistic previously accumulatedsince the discovery of cosmic rays one century ago!
AMS collected more than 17 billion eventsN
events ~ 46 106 / day
![Page 9: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/9.jpg)
I – Science case1. Galactic Cosmic Rays2. AMS02
II – Collaboration LAPP/LAPTh/LPSC1. Teams and context2. Support asked for the project
III – Conclusions
![Page 10: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/10.jpg)
Sylvie ROSIER-LEESAMS-France
AMS-02 group @ LAPP
Pierre SALATIAstroparticle group @ LAPTh
Laurent DEROMEAMS-02 group @ LPSC
- e- and e+ fluxes (ECAL)- Dark matter
- Propagation- Dark matter
Team - 1 ½ CNRS- 1 émérite- 1 ½ MdC/Prof.- 1 post-doc
- 1 CNRS- 2 Prof.- 1 PhD
- 5 CNRS- 2 émérites- 1 post-doc- 1 PhD
- Nuclear fluxes (RICH)- Propagation + GreAT- Dark matter
Collaboration LAPP/LAPTh/LPSC
“Science”
ANR USINE-CRYPTIC (JCJC 2011) + ANR GCRPAE (blanc 2012) => USINE project
(overlap with DMastro, see Geneviève's talk)
P. Brun, J. Pochon (PhD)A. Fiasson (Post-doc)=> several papers
A. Barrau, L. Derome, D. Maurin, P. Salati, R. Taillet => ~ 15 papers (since 2001)
![Page 11: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/11.jpg)
Sylvie ROSIER-LEESAMS-France
AMS-02 group @ LAPP
Pierre SALATIAstroparticle group @ LAPTh
Laurent DEROMEAMS-02 group @ LPSC
- e- and e+ fluxes (ECAL)- Dark matter
- Propagation- Dark matter
Team
Collaborations
- 1 ½ CNRS- 1 émérite- 1 ½ MdC/Prof.- 1 post-doc
- 1 CNRS- 2 Prof.- 1 PhD
- 5 CNRS- 2 émérites- 1 post-doc- 1 PhD
- Nuclear fluxes (RICH)- Propagation + GreAT- Dark matter
Collaboration LAPP/LAPTh/LPSC
“Science”
ANR USINE-CRYPTIC (JCJC 2011) + ANR GCRPAE (blanc 2012) => USINE project
(overlap with DMastro, see Geneviève's talk)
AMS-01 (1998) +02 (2011-XX)=> 5 meetings since launch P. Brun, J. Pochon (PhD)
A. Fiasson (Post-doc)=> several papers
A. Barrau, L. Derome, D. Maurin, P. Salati, R. Taillet => ~ 15 papers (since 2001)
![Page 12: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/12.jpg)
ANR Project – 2010 (JCJC)
=> Rejected...
![Page 13: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/13.jpg)
ANR Project – 2011 (blanc)
=> Rejected...
![Page 14: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/14.jpg)
ANR project: tasks and objectives
LPSC + LAPTh+ LAPP
LPSC
LAPP
LPSC + LAPTh
![Page 15: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/15.jpg)
USINE (in progress)(http://lpsc.in2p3.fr/usine)
![Page 16: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/16.jpg)
USINE
(http://lpsc.in2p3.fr/usine)
+ regular meetings (LAPP/LAPTh/LPSC)
✔ USINE 1 (02/12/2010) : http://indico.in2p3.fr/conferenceDisplay.py?confId=4728✔ USINE 2 (24/02/2011) : http://indico.in2p3.fr/conferenceDisplay.py?confId=5152✔ USINE 3 (22/06/2011) : http://indico.in2p3.fr/conferenceDisplay.py?confId=5590✔ USINE 4 (14/12/2011) : http://indico.in2p3.fr/conferenceDisplay.py?confId=6112
Access key: dark
USINE (in progress)
![Page 17: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/17.jpg)
Conclusions
Big time with AMS-02!
Strong existing synergy between 3 ENIGMASS labs![we work together, we sometimes fail, but we mostly succeed!]
- AMS regular meetings since launch- Phenomenology 'USINE' regular meetings
=> Strong collaboration since 1998 (involving several researchers from each team)
ENIGMASS post-docs would be greatly appreciated![ANR projects failed, SMINGUE post-doc ranked 1st but not attributed...]
N.B.: we have a highly recommended post-doc candidatein store who wishes to work with us
... and we have plenty of nice studies to carry on!=> Profile for the post-docs: modelling and data analysis
![Page 18: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/18.jpg)
Dos-dessus
![Page 19: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/19.jpg)
Adapted from Moskalenko et al. (2004)AMS, CREAM, PAMELA
ANTARES
km3
FERMI, AMS-γ
AMS GAPS
d_
HESS
νν−
Cosmic Ray journey in 3 steps: 1. Synthesis and acceleration 2. Transport (diffusion & interactions) 3. Solar modulation+detection
1
2
3
=> Use LiBeB to calibrate the transport coefficients
=> Search for DM where “standard” production is rare (secondary)
From sources to detect ion: modell ingthe astrophysical 'backgrounds '
![Page 20: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/20.jpg)
Time at location [s]
DAQ efficiency
Acquisition rate [Hz]
Particle rates vary from200 to 2000 Hz per orbit
On average:DAQ efficiency 85%DAQ rate ~700Hz
Orbital DAQ parameters
![Page 21: Galactic CosmicRay Propagation in the AMS02 Era](https://reader036.vdocuments.net/reader036/viewer/2022062513/62b218f44b7ffb3a272a27f4/html5/thumbnails/21.jpg)
Timeline